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dc.contributor.authorZapartas, E.
dc.contributor.authorMink, S. E. de
dc.contributor.authorVan Dyk, Schuyler D.
dc.contributor.authorFox, O. D.
dc.contributor.authorSmith, N.
dc.contributor.authorBostroem, K. A.
dc.contributor.authorKoter, A. de
dc.contributor.authorFilippenko, A. V.
dc.contributor.authorIzzard, R. G.
dc.contributor.authorKelly, P. L.
dc.contributor.authorNeijssel, C. J.
dc.contributor.authorRenzo, M.
dc.contributor.authorRyder, S.
dc.date.accessioned2017-07-27T18:37:59Z
dc.date.available2017-07-27T18:37:59Z
dc.date.issued2017-06-22
dc.identifier.citationPredicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002ap 2017, 842 (2):125 The Astrophysical Journalen
dc.identifier.issn1538-4357
dc.identifier.doi10.3847/1538-4357/aa7467
dc.identifier.urihttp://hdl.handle.net/10150/624948
dc.description.abstractMany young, massive stars are found in close binaries. Using population synthesis simulations. we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type. Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star > 8-10 M., ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially. 23 M.. Although unlikely (< 1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broadlined Type. Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern. the evolution of SN progenitors.
dc.description.sponsorshipNASA [NAS 5-26555]; NASA from STScI [GO-14075, AR-14295]; Netherlands Research School for Astronomy (NOVA); Marie Sklodowska-Curie Action (H MSCA-IF, project BinCosmos) [661502]; Christopher R. Redlich Fund; TABASGO Foundation; NSF [AST-1211916, AST-1312221, AST-1515559]; STFC [ST/L003910/1]; Churchill College, Cambridgeen
dc.language.isoenen
dc.publisherIOP PUBLISHING LTDen
dc.relation.urlhttp://stacks.iop.org/0004-637X/842/i=2/a=125?key=crossref.6de6379577b8073c09ff49397a973ebfen
dc.rights© 2017. The American Astronomical Society. All rights reserved.en
dc.rights.urihttp://rightsstatements.org/vocab/InC/1.0/
dc.subjectbinaries: closeen
dc.subjectbinaries: generalen
dc.subjectstars: evolutionen
dc.subjectstars: massiveen
dc.subjectsupernovae: generalen
dc.subjectsupernovae: individual (SN 2002ap)en
dc.titlePredicting the Presence of Companions for Stripped-envelope Supernovae: The Case of the Broad-lined Type Ic SN 2002apen
dc.typeArticleen
dc.contributor.departmentUniv Arizona, Steward Observen
dc.identifier.journalThe Astrophysical Journalen
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en
dc.eprint.versionFinal published versionen
refterms.dateFOA2018-09-11T21:47:53Z
html.description.abstractMany young, massive stars are found in close binaries. Using population synthesis simulations. we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type. Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star > 8-10 M., ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially. 23 M.. Although unlikely (< 1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broadlined Type. Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern. the evolution of SN progenitors.


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